keywords:Kuiper beltdebris disks

imaging of extrasolar planetsorbit-orbit resonance

Planetary Dynamics at the Outer Limits

E. ChiangUC Berkeley

Sample Blinking

Sample Blinking

KBOs = test particles

M ~ 0.1 M⊕

3 AU-3 π (100 km)2 1 km s-1

conjunction

Neptune-Pluto Orbit-Orbit Resonance

“resonant width” Δ a resb

2.9:2

3:2 3:2

3.1:2

2.9:2

3:2

Resonant KBOs (~26%)

Orbital Migration by Planetesimal Ejection

Resonance Sweeping

Plutino (3:2) Snapshot

Wave pattern rotates rigidly with Neptune

2:1 = Planetary Speedometer

tmigrate = 106 yrtmigrate ≡ a/(da/dt) ≥ 107 yr

Big KBOs are excited

The Kuiper Belt: The Global View

678130 AU67880 AU

678

70 AU

planetary wire(secular approximation)

closed non-crossing orbits

Eccentric planet begetseccentric ring

Equilibrium belt orbitsare eccentric

and aligned withthe planet’s orbit

Fomalhaut

planetary wire(secular approximation)

closed non-crossing orbits

Dissipative relaxation of parent bodies

onto non-crossing (forced eccentric)

orbits

Relaxation occurs during:

• Present-day collisional cascade

• Prior coagulation

Wyatt et al. 99Kalas et al. 05

eforced(a) =b(2)3/2(aplanet/a)

b(1)3/2(aplanet/a)

eplanet

J SU

N

Lecar et al. 2001

Surface brightnessfrom Kalas et al. 05

Constraining ap and Mp

using the sharp inner belt edge

Inner belt edge =Outer edge of planet’s

“chaotic zone”

Chaotic zone width ~ (Mplanet/Mstar)2/7 aplanet

chaotic zone

m:m

−1

m+

1:m

∆s

x

Planetary chaotic zone

= Region where first-orderresonances overlap

∆x

conjunction #1

#2

#3

#1

Regular

Chaotic

Wisdom 1980Duncan et al. 1989

Quillen 2006#2

#3

Cha

otic

zon

e Chaotic zone

. . .

Randomwalk

in aand e

Orbit crossingand ejection

J SU

N

Lecar et al. 2001

Surface brightnessfrom Kalas et al. 05

Constraining ap and Mp

using the sharp inner belt edge

Inner belt edge =Outer edge of planet’s

“chaotic zone”

Chaotic zone width ~ (Mplanet/Mstar)2/7 aplanet

chaotic zone

not thermal emission from planetary atmosphere

40 RJ reflective dust disk?

Variable Hα emission?

not confirmed: only 2 epochs

Candidate planet (0.5 Jupiter mass)

HR 8799A-type star 30-60 Myr oldwith 4 Super-Jupiters

Orbital resonances afford stabilityd:c = 2:1 resonance

Other possibilities included:c:b = 4:2:1e:d:c = 4:2:1

dynamical masses < 20 Jupitermasses each

log(

L/L

!)

log(age/yr)

6-7MJ

7-10MJ

Cloudy spectra unlikebrown dwarfs

Gemini Planet Imager (GPI)2012

Pan-STARRS (once a week, mag 24)

and LSST (once every few days, mag 24.5)

PS1

LSST site

Deriving the chaotic zone width

Resonance overlap

m:m

−1

m+

1:m

∆s

x

∆s

a

∼

(

x

a

)2

Resonance spacing

then chaos

if ∆x > ∆s

i.e., if x <

(

Mp

M∗

)2/7

a

∆x

Deriving the chaotic zone widthI. The kick at conjunction

ap

Mp

x

Ωp

= ap + x

a

2x

∆x

∆e ∼

∆v

v∼

1

v

GMp

x2∆t

∼

Mp

M∗

(

a

x

)2

x ! a

Kick in eccentricity

Kick in semimajor axis

Use Jacobi constant: CJ ≈ −GM∗

2(a + x)− Ωp

√

M∗(a + x)(1 − e2)

⇒x∆x

a2∼ (∆e)2 ⇒

∆x

a∼

(

Mp

M∗

)2(

a

x

)5

∆e

∆x

eplanet = 0.12

ωplanet = ωbelt (nested ellipses)

aplanet = 115 AU

e.g., if

then

Mplanet = 0.5MJ

Mbelt > Mparent bodies ∼ 3M⊕

Enough material forgas giant core

Asymmetric capture:Migration-shifted potentials

Φ

“V”

π

Direct

Indirect

∆Φ ∼

t2librate

torbitaltmigrate

Results

If Mplanet ↑ then aplanet ↓

Planet position too farfrom dust belt

→ Mplanet < 3 MJ

Planet also evacuatesKirkwood-type gaps

Chiang et al. 2008Kalas et al. 2008

10

100

10000.3 MJ 6:5

11:95:4

9:74:3

10

100

Num

ber

of st

able

par

ent b

odie

s (in

0.1

AU

bin

s)

1 MJ

4:3 7:5

10

100

3 MJ

3:2

90 100 110 120 130 140 1501

10

100

Time-averaged semimajor axis (AU)

10 MJ

5:37:4

∴

Results

Surface brightnessprofiles broaden too much

If Mplanet ↑ then edust ↑

→ Mplanet < 3 MJ

100 120 140 160 180 200Semimajor axis a (AU)

0.0

0.2

0.4

0.6

0.8

1.0

Rel

ativ

e

K05 model0.1 MJ, apl=120 AU0.3 MJ, apl=115.5 AU1 MJ, apl=109 AU3 MJ, apl=101.5 AU10 MJ, apl=94 AU

∴

Mbelt > Mparent bodies ∼ 3M⊕

Enough material for gas giant core

eplanet = 0.12

ωplanet = ωbelt (nested ellipses)

aplanet = 115 AU

e.g., if

then

Mplanet = 0.5MJ

• The Kuiper belt comprises tens of thousands of icy, rocky objects having sizes greater than 100 km

• Many KBOs occupy highly eccentric and inclined orbits that imply a violent past

• Pluto and other Resonant KBOs share special gravitational relationships with Neptune

• Extrasolar debris disks are nascent Kuiper belts

• Belts are gravitationally sculpted by planets

Fomalhaut b: Planet-Debris Disk Interaction

Step 1: Screen parent bodies for gravitational stability

tage ∼ 108 yr

t = 0Myrt = 100Myr

chaoticwidth

Step 2: Replace parent bodies with dust grains

Step 3: Integrate dust grains with radiative force for collisional lifetime

tcollision ∼ torb/τ ∼ 0.1 Myr

∆t = tcollision = 0.1 Myr

Classical

Excited

1000 100 10 1

20 25 30 35-4

-2

0

2

4

6

mR

Nominal Diameter at 42 AU (km)

log

N(<

mR)

(de

g-2 )

Measured Extrapolated

Parent bodies collide once in system age

Most visible grains are just largeenough to avoid stellar blow-out

Collisional Cascade

Distribution of sizes ofKuiper belt objects

Results

If Mplanet ↑ then aplanet ↓

Planet position too farfrom dust belt

→ Mplanet < 3 MJ

Planet also evacuatesKirkwood-type gaps

Chiang et al. 2008Kalas et al. 2008

10

100

10000.3 MJ 6:5

11:95:4

9:74:3

10

100

Num

ber

of st

able

par

ent b

odie

s (in

0.1

AU

bin

s)

1 MJ

4:3 7:5

10

100

3 MJ

3:2

90 100 110 120 130 140 1501

10

100

Time-averaged semimajor axis (AU)

10 MJ

5:37:4

∴

Mbelt > Mparent bodies ∼ 3M⊕

Enough material for gas giant core

M∗ = 1M"

M∗ = 10M"

M∗ = 102M"

M∗ = 103M"

Measuring Debris Disk Masses

N

ssblow

∼ 0.2µm

svisible ssubmm stop

dN/ds ∝ s−q

850 µm flux consistent w/

q = 7/2(Dohnanyi)

[from tcollision(stop) ∼ tage]

stop ∼ 10 cm

∼ 100 µm

MSED(stop) ∼ 0.01M⊕

Packed planetary systems

Packedformation

Instabilityand ejection

occurs whenplanets outweigh

parent disk

Stabilityrestored

Regularizationby dynamical

friction

Signature recorded in Kuiper belt

Numerical simulations of packed planetary systems

Solar system-like outcomes emerge from chaos

Dynamical friction:Small bodies slow

big bodies

Stirringof KBOs

byRogue

Ice Giants

ObservedSimulated

Short-Period Comets

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l

Raising Sedna’s Periby Stellar Encounters

Typical opencluster

Before After

Fernandez & Brunini 00

Praesepe cluster M44

· n∗ ∼ 4 stars/pc3 (R1/2 ∼ 2 pc)

· t ∼ 200 Myr

· 〈v2

∗〉1/2 ∼ 1 km/s

Discovery ofKuiper Belt Object

(KBO) #3

1992 QB1: “Smiley”

David Jewitt (U Hawaii)Jane Luu (UC Berkeley)

Size depends on observed brightness and intrinsic reflectivity (albedo)

IxionQuaoar

Planetary Protection Mechanism:Orbit-Orbit Resonance

Neptune makes 3 orbits

for every

2 orbits of Pluto

“Dance of the Plutinos”

The Orbit of Sedna

Resonant KBOs

5:1 4:1 3:1 5:2 7:3 2:1 9:5 7:40

6

12Number

5:3 8:5 3:2 10:7 7:5 11:8 4:30

40

80

Number

13:10 9:7 14:11 5:4 11:9 6:5 1:1036

Number

2003 UB313 (mapp = 19)Diameter = 2397±100 km

vs.

PlutoDiameter = 2274 km

Palomar 48-inch / M. Brown, C. Trujillo, & D. Rabinowitz (Caltech, Yale)

Hubble Space Telescope

2003 UB313

“Xena”Bigger than Pluto

“Santa”

“Easter Bunny”

I.A.U. definition

(a) orbits the Sun(b) hydrostatic (round) shape(c) not a satellite(d) not cleared its

neighborhood

“Dwarf Planets”

Nix

Hydra

• The Kuiper belt comprises tens of thousands of icy, rocky objects having sizes greater than 100 km

• The Kuiper belt is the source of short-period comets

• Pluto and other Resonant KBOs share special gravitational relationships with Neptune

• Many KBOs, especially large ones, occupy highly eccentric and inclined orbits that imply a violent past

• Other star systems have their own Kuiper belts

What we know:

1 “Large” Neptune Trojan in 60 °~10-30 Large Neptune Trojans

vs. ~1 Large Jovian Trojan

(“Large” ≡ 130-230 km diameterassuming 12-4% visual albedo)

⇒

First discovered Neptune Trojan (1:1)

Neptune

based on Mike Brown’s survey limits:1 Earth mass at less than 200 AU1 Neptune at less than 500 AU

1 Jupiter (in reflected light) at less than 1000 AU

based on Hipparcos and Tycho-2cannot be a self-luminous main-sequence star above

the hydrogen burning limit

infrared detection of a Jupiter or brown dwarfcould be interesting

daughter dust particle

birth ring

Theoretical Snapshots of Resonant KBOs

•

•

Chiang & Jordan 2002

⇐ Plutinos 3:2

Twotinos 2:1 ⇒

Observational Facts and Theoretical Deductions

1. Pluto is the largest known member of a swarm of billions of outer solar system bodies that supply

new comets.2. Pluto and the Plutinos are locked in an orbital

resonance established by Neptune.3. The orbits of many Kuiper Belt Objects are dynamically

excited.4. Pluto is not alone in having an

orbital companion.

Pluto Charon 1999 TC 36